Kepler-296 is a binary star system with two M-dwarf components separated by 0.2 ” .
Five transiting planets have been confirmed to be associated with the Kepler-296 system ; given the evidence to date , however , the planets could in principle orbit either star .
This ambiguity has made it difficult to constrain both the orbital and physical properties of the planets .
Using both statistical and analytical arguments , this paper shows that all five planets are highly likely to orbit the primary star in this system .
We performed a Markov-Chain Monte Carlo simulation using a five transiting planet model , leaving the stellar density and dilution with uniform priors .
Using importance sampling , we compared the model probabilities under the priors of the planets orbiting either the brighter or the fainter component of the binary .
A model where the planets orbit the brighter component , Kepler-296A , is strongly preferred by the data .
Combined with our assertion that all five planets orbit the same star , the two outer planets in the system , Kepler-296 Ae and Kepler-296 Af , have radii of 1.53 \pm 0.26 and 1.80 \pm 0.31 R _ { \oplus } , respectively , and receive incident stellar fluxes of 1.40 \pm 0.23 and 0.62 \pm 0.10 times the incident flux the Earth receives from the Sun .
This level of irradiation places both planets within or close to the circumstellar habitable zone of their parent star .